## For a detailed analysis of stellar chemical abundances, high-resolution spectra in the optical have mainly been used, while the development of near-infrared (NIR) spectrograph has opened new wavelength windows.

Fe i Lines in 0.91–1.33 μm Spectra of Red Giants for Measuring the Microturbulence and Metallicities

## Multiple codes are available to derive atmospheric parameters and individual chemical abundances from high-resolution spectra of AFGKM stars.

Modern stellar spectroscopy caveats

## We have used high resolution spectra obtained with HARPS-N@TNG for HD 344787 and the more famous Polaris DCEP, to infer their detailed chemical abundances.

HD 344787: a true Polaris analogue?

## Detailed chemical abundances of light elements as well as heavy neutron-capture elements have been determined for our 22 stars.

R-process-rich Stellar Streams in the Milky Way* * This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.

## Precise chemical abundances allow us to confront the theoretical yields for AGB stellar masses and metallicities expected at the bright end of the PNLF.

On the most luminous planetary nebulae of M31

## Context: Precise chemical abundances coupled with reliable ages are key ingredients to understand the chemical history of our Galaxy.

Abundance–age relations with red clump stars in open clusters

## We present chemical abundances for 21 elements (from Li to Eu) in 150 metal-poor Galactic stars spanning −4.

High-resolution spectroscopic follow-up of the most metal-poor candidates from SkyMapper DR1.1

## We present chemical abundances for the elements carbon, sodium, and fluorine in 15 red giants of the globular cluster M4, as well as six red giants of the globular cluster ω Centauri.

Fluorine Abundances in the Globular Cluster M4

## In order to make progress on these issues, its important to collect high-resolution spectroscopic data to determine their fundamental parameters and individual chemical abundances.

HERMES spectroscopy of normal A and Am stars

## For the brightest RVS targets, stellar atmospheric parameters and individual chemical abundances are automatically estimated by the Generalized Stellar Parametriser spectroscopy group (GSP-Spec).

GSP-spec line list for the parametrisation of Gaia-RVS stellar spectra

## We derived chemical abundances of carbon from two atomic lines for 757 FGK stars in the HARPS-GTO sample, observed with high-resolution (R ∼ 115000) and high-quality spectra.

Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program. IV. Carbon and C/O ratios for Galactic stellar populations and planet hosts

## However the derived chemical abundances do not show significant indications of mixing when adopting baseline values typical for the system environment.

Clues on the Origin and Evolution of Massive Contact Binaries: Atmosphere Analysis of VFTS 352

## For a detailed analysis of stellar chemical abundances, high-resolution spectra in the optical have mainly been used, while the development of near-infrared (NIR) spectrograph has opened new wavelength windows.

Fe i Lines in 0.91–1.33 μm Spectra of Red Giants for Measuring the Microturbulence and Metallicities

## As is the case for the one other galaxy dominated by $r$-process enhanced stars, Reticulum II, Tucana III's stellar chemical abundances are consistent with pollution from ejecta produced by a binary neutron star merger, although a different $r$-process element or dilution gas mass is required to explain the abundances in these two galaxies if a neutron star merger is the sole source of $r$-process enhancement.

Chemical abundance analysis of tucana III, the second r-process enhanced ultra-faint dwarf galaxy

## Among them, the ionizing stellar populations and the gas geometry make the recipes designed to derive chemical abundances from nebular emission lines to differ from those calibrated in the Local Universe.

Extreme emission-line galaxies in SDSS – I. Empirical and model-based calibrations of chemical abundances

## We model the stellar continuum to derive chemical abundances and measure gas-phase abundances with standard nebular diagnostics.

A comparison of stellar and gas-phase chemical abundances in dusty early-type galaxies

## The Open Cluster Chemical Abundances from Spanish Observatories (OCCASO) survey aims to complement all this work by determining OCs accurate radial velocities and chemical abundances from high-resolution, R≥60 000, spectra.

OCCASO IV. Radial velocities and open cluster kinematics

## The study of open-cluster chemical abundances provides insights on stellar nucleosynthesis processes and on Galactic chemo-dynamical evolution.

OCCASO III. Iron peak and $\alpha$ elements of 18 open clusters. Comparison with chemical evolution models and field stars

## For the 13 newly identified HgMn stars we derived photospheric chemical abundances by spectral synthesis.

Discovery of new mercury–manganese stars, including a fast rotator

## We used the photospheric chemical abundances of Asplund et al.

The EUV spectrum of the Sun: Quiet- and active-Sun irradiances and chemical composition

## We found that the CO/H2O mixing ratio of 2I/Borisov changed drastically before and after perihelion, indicating the heterogeneity of the cometary nucleus, with components formed at different locations beyond the volatile snow-line with different chemical abundances.

Compact pebbles and the evolution of volatiles in the interstellar comet 2I/Borisov

## To explore the metallicity-dependence of mass loss we calculate model grids at three different chemical abundances.

Carbon star wind models at solar and sub-solar metallicities: a comparative study: I. Mass loss and the properties of dust-driven winds

## Shallower metallicity gradients derived from HII regions produce unreasonably large corrections, suggesting that the use of chemical abundances derived from such tracers as a proxy for Cepheid metallicity is unreliable.

The Cepheids of M33 : distance and metallicity effects through Sloan filters

## This new FLAMES sample offers a sufficiently large number of stars with chemical abundances derived at high accuracy to firmly establish the existence of a plateau in [$\alpha$/Fe] at $\sim 0. The chemical evolution of the dwarf Spheroidal galaxy Sextans 10.1051/0004-6361/201730931 ## Chemical abundances in the X-ray halos (also known as the intracluster medium, ICM) of clusters and groups of galaxies can be measured via prominent emission line features in their X-ray spectra. Nitrogen abundance in the X-ray halos of clusters and groups of galaxies 10.1051/0004-6361/201935162 ## We study the mass-size plane of galaxies in cosmological hydrodynamical simulations, as a function of velocity dispersion, age, chemical abundances, ellipticity and spin parameters with the aim at assessing to what extent the current cosmological paradigm can reproduce these observations and provide a physical interpretation of them. The mass-size plane of EAGLE galaxies 10.1051/0004-6361/201833750 ## Currently, observations show that the presence of planetary companions is closely linked to the metallicity and the chemical abundances of the host stars. Chemical composition of planet building blocks as predicted by stellar population synthesis ## which are caused by bimodal populations in age and/or chemical abundances, eMSTOs are believed to be owing to stellar rotation. Stellar rotation and the extended main sequence turnoff in the open cluster NGC 5822 10.1051/0004-6361/201935177 ## On the other hand, the mean spectrum was fit with spectral synthesis to derive atmospheric parameters and chemical abundances. HD 96446: a long-period binary with a strongly magnetic He-rich primary with β Cephei pulsations ## In clusters of galaxies, the red sequence is believed to be a consequence of a correlation between stellar mass and chemical abundances, with more massive galaxies being more metal-rich and, as a consequence, redder. On the Origin of the Scatter in the Red Sequence: An Analysis of Four CLASH Clusters 10.1038/s41586-018-0826-3 ## Using spectral synthesis models developed for SN 2017iuk, we show that these features are characterized by chemical abundances that differ from those observed in the ejecta of SN 2017iuk at later times. Signatures of a jet cocoon in early spectra of a supernova associated with a γ-ray burst 10.1051/0004-6361/201935772 ## Although there have been numerous studies of chemical abundances in the Galactic bulge, the central two degrees have been relatively unexplored due to the heavy and variable interstellar extinction, extreme stellar crowding, and the presence of complex foreground disk stellar populations. The inner two degrees of the Milky Way. Evidence of a chemical difference between the Galactic Center and the surrounding inner bulge stellar populations 10.1051/0004-6361/201936125 ## Using ESO VLT/FLAMES spectra, we measure the chemical abundances of Y, Ba, La, Nd, and Eu, in 98 stars covering$-2.

Neutron-capture elements in dwarf galaxies I: Chemical clocks & the short timescale of the $r$-process

## Spectra emitted from ionized nebulae typically contain collisionally excited and recombination lines, which can be used to trace physical conditions and chemical abundances of the interstellar medium in our Galaxy and other galaxies.

AtomNeb: IDL Library for Atomic Data of Ionized Nebulae

## Using the Modules for Experiments in Stellar Astrophysics code and considering the effects of WD's mass, mass-accretion rate and the chemical profiles of WD which are described by new parameter --- mixing depth on the chemical abundances of nova ejecta, we investigate the possibility that bimodal dust species are produced in a nova eruption.

The formation of bimodal dust species in nova ejecta – I. Chemical conditions

## We can now measure the chemical abundances in those old stars, which is similar to a genetic fingerprint that allows us to identify the parents.

Evolving stellar models to find the origins of our galaxy

10.1051/0004-6361/201835004

## We determined the main atmospheric parameters, kinematic properties, orbital parameters, and stellar ages for 109 newly observed stars and chemical abundances of 23 chemical species for 249 F, G, and K dwarf stars observed in the present study and in our previous study.

High-resolution spectroscopic study of dwarf stars in the northern sky: Na to Zn abundances in two fields with radii of 20 degrees⋆,⋆⋆

10.1134/S1063773719050050

## As a result, among the galaxies of its class Bootes I now has the largest sample of stars (11) with a homogeneous set of atmospheric parameters and chemical abundances, and this makes it the most promising for studying the chemical evolution of UFD galaxies.

Contribution of type Ia supernovae to the chemical enrichment of the ultra-faint dwarf galaxy Bootes I

## Chemical abundances of eight different elements were obtained.

High-resolution spectroscopy of the high-velocity hot post-AGB star IRAS 18379–1707 (LS 5112)

## In our work we obtained the stellar parameters and chemical abundances of 24 elements (O, Na, Mg, Al, Si, Ca, Ti, V, Cr, Mn, Fe, Co, Sc, Ni, Cu, Zn, Y, Zr, Ba, La, Ce, Eu, Nd and Dy).

Chemical evolution of the metal-poor globular cluster NGC 6809

10.1038/s41586-019-1789-8

## Observations of an accretion disk around a hot white dwarf star reveal that the chemical abundances in its disk are similar to those thought to exist deep in icy giant planets, so the white dwarf must be accreting a giant planet.

Accretion of a giant planet onto a white dwarf star

## Chemical abundances were determined from the spectra for 40 stars of the sample.

The Pristine survey – V. A bright star sample observed with SOPHIE

## As far as the p-capture elements are concerned, the chemical abundances are typical of 1G stars, as expected from the location of our targets in the ChM.

Chemical abundances along the 1G sequence of the chromosome maps: The Globular Cluster NGC 3201.

10.1051/0004-6361/201834729

## We estimated the spectroscopic contamination level, $\textit{v sin i}$, activity, stellar parameters and chemical abundances for 249 of the most promising targets.

Catalog for the ESPRESSO blind radial velocity exoplanet survey

## We presented distributions of chemical abundances in the $V_{\phi}$ versus \textit{R} coordinate.

Elemental Abundance Distributions in the (R, V ϕ ) Plane with LAMOST DR5 and Gaia DR2

## Furthermore, by combining them, a better constraint might be attained for star formation history and chemical abundances of subpopulations in GCs.

Multiple populations in globular clusters: Unified efforts from stellar evolution and chemical evolution models

## The exploration of the spatial distribution of chemical abundances in star-forming regions in galactic discs provides clues to understand the complex interplay of physical processes that regulate the star formation activity and the chemical enrichment across a galaxy.

Azimuthal variations of oxygen abundance profiles in star-forming regions of of disc galaxies in the EAGLE simulations

10.1051/0004-6361/201936109

## Our objective is also to characterise its seven evolved stars by deriving their atmospheric parameters and chemical abundances.

A comprehensive study of NGC 2345, a young open cluster with a low metallicity

## Shallower metallicity gradients derived from HII regions produce unreasonably large corrections, suggesting that the use of chemical abundances derived from such tracers as a proxy for Cepheid metallicity is unreliable.

The Cepheids of M33 : distance and metallicity effects through Sloan filters

10.1051/0004-6361/201935234

## A wide spread of chemical abundances within the Arcturus stream indicates that the group is not a dissolved open cluster.

Disentangling the Arcturus stream

10.1051/0004-6361/201936687

## For the remaining single stars we derived the stellar parameters, extinction, radial and projected rotational velocities, and chemical abundances for 21 species with atomic number up to 40.

Stellar population astrophysics (SPA) with the TNG. Characterization of the young open cluster ASCC 123

10.1051/0004-6361/201936978

## We compare differential abundances of several stars from the Hyades and Praesepe tails: the stars that differ more in chemical abundances also have distinct kinematics, even though they have been identified as members of the tail.

Differential abundances of open clusters and their tidal tails: chemical tagging and chemical homogeneity

10.1017/S1743921318007408

## Planetary nebulae (PNe) are oldand intermediate-age star remnants and their chemical abundances can be obtained up to 3-4 Mpc.

What do planetary nebulae and H II regions reveal about the chemical evolution of nearby dwarf galaxies?

10.5303/JKAS.2019.52.3.57

## We present an analysis of the chemical abundances and kinematics of six low-mass dwarf stars, previously claimed to be candidate hypervelocity stars (HVSs).

Origin and Status of Low-Mass Candidate Hypervelocity Stars

10.1051/0004-6361/201937343

## To this end, we study the spectral energy distribution of LS V+22 25 and perform a quantitative spectroscopic analysis that includes the determination of chemical abundances for He, C, N, O, Ne, Mg, Al, Si, S, Ar, and Fe.

A stripped helium star in the potential black hole binary LB-1.

## We find that the method works very well in disk midplane and surfaces regions, where approximately 20-30 gas phase species, connected by $\sim$50-60 gas phase reactions, are sufficient to reproduce the targeted ionization fraction and chemical abundances.

Chemical Network Reduction in Protoplanetary Disks

10.1134/S1990341319030040

## Using the model atmosphere method, we determined the fundamental parameters and chemical abundances in the atmosphere approving the status of a post-AGB star for V1648 Aql.

Optical spectrum of distant OH/IR star V1648 Aql (IRAS 19386+0155)

## First, we find that a combination of models with minimal assumptions and broadband transmission spectra with current facilities allow precise estimates of chemical abundances.

On degeneracies in retrievals of exoplanetary transmission spectra

## A key difference between the 1D and 2D models is in the chemical abundances.

The first multidimensional view of mass loss from externally FUV irradiated protoplanetary discs

## Omega Cen can be classified as an extreme Type II GC, with a ChM displaying three main streams, each with its own variations in chemical abundances.

The Hubble Space Telescope UV Legacy Survey of Galactic Globular Clusters – XIX. A chemical tagging of the multiple stellar populations over the chromosome maps

## Chemical abundances and abundance ratios measured in galaxies provide precious information about the mechanisms, modes and time scales of the assembly of cosmic structures.

The evolution of CNO isotopes: the impact of massive stellar rotators

## The chemical abundances demonstrate that both systems are clearly galaxies and not globular clusters.

Detailed Abundances in the Ultra-faint Magellanic Satellites Carina II and III.

10.1051/0004-6361/201834554

## We used a non-NLTE analysis in a self-consistent semi-automatic routine based on TLUSTY and SYNSPEC to determine atmospheric parameters and chemical abundances.

Radial abundance gradients in the outer Galactic disk as traced by main-sequence OB stars.

10.1051/0004-6361/201935369

## Here, we verify the large N overabundance of 2M12451043+1217401 and re-determined the chemical abundances for a wider range of chemical species, including light and heavy elements.

Discovery of a nitrogen-enhanced metal-poor binary system: Possible evidence for pollution from an extinct massive AGB Star

10.1038/s41550-019-0904-y

## To what extent do small-scale processes, such as star formation and black-hole accretion, affect global galaxy properties such as stellar masses, star formation rates and chemical abundances?.

Feedback and its role in galaxy formation

## We examine the chemistry, kinematics, and dynamics of this metal-rich halo sample using chemical abundances and radial velocities provided by the fourteenth APOGEE data release (DR14) and proper motions from the second Gaia data release (DR2).

The metal-rich halo tail extended in |z|: a characterization with Gaia DR2 and APOGEE

10.22201/ia.01851101p.2019.55.02.13

## Galactocentric radii and chemical abundances were collected from the literature, carefully selecting a homogeneous sample for each galaxy.

Metallicity Gradients in M 31, M 33, NGC 300 and the Milky Way Using Abundances of Different Elements

## We segment this predominantly photoionised region of study into elliptical annuli on the basis of the H$\alpha$ flux distribution to study the variation of chemical abundances and their ratios, and find no significant chemical variation.

Small-scale chemical abundance analysis in a blue compact dwarf galaxy SBS 1415+437

## While the innermost halo and Gaia Enceladus regions have chemical abundances consistent with high- and low-$\alpha$ populations in the halo, respectively, chemical abundances of stars in the high-energy retrograde halo are different from the two populations; their [{X}/{Fe}], where X represents Na, Mg, and Ca, are even lower than those in Gaia Enceladus.

Origin of the excess of high-energy retrograde stars in the Galactic halo